Why is Rotation Speed Proportional to Mass? mv 2 /R = GMm/R 2 ; centrifugal force = gravitational force due to the mass “M” within the radius “R.” =>

Slides:



Advertisements
Similar presentations
Astronomy Class Notes Jim Mims.
Advertisements

MEASURING DISTANCES IN ASTRONOMY Basic Principles: Geometric methods Standard candles Standard rulers [the last two methods relate quantities that are.
Introduction to Astrophysics Lecture 14: Galaxies NGC1232.
Distances to Astronomical Objects
Astronomical distances The SI unit for length, the meter, is a very small unit to measure astronomical distances. There units usually used is astronomy:
How Far is far ? Measuring the size of the Universe.
Astronomical Distances Distances in astronomy are huge The Moon is 240,000 miles away The Sun is 93, 000,000 miles away Neptune is 2,810,687,500 miles.
Distances to Astronomical Objects. Recap Distances in astronomy – Measuring distances directly with light travel time – Measuring distances geometrically.
OPTION E - ASTROPHYSICS E3 Stellar distances Parallax method
Chapter 20 Dark Matter, Dark Energy, and the Fate of the Universe.
Charles Hakes Fort Lewis College1. Charles Hakes Fort Lewis College2.
Angles Angle  is the ratio of two lengths:
The Life Cycles of Stars and our Sun. Your Questions 1.Have you ever heard of the sun song by the group They Might be Giants?
PRESENTATION TOPIC  DARK MATTER &DARK ENERGY.  We know about only normal matter which is only 5% of the composition of universe and the rest is  DARK.
© 2010 Pearson Education, Inc. Chapter 22 Dark Matter, Dark Energy, and the Fate of the Universe.
Rotational Motion and The Law of Gravity
Copyright © 2010 Pearson Education, Inc. Clicker Questions Chapter 10 Measuring the Stars.
Universe Eighth Edition Universe Roger A. Freedman William J. Kaufmann III CHAPTER 24 Galaxies Galaxies.
GALAXIES, GALAXIES, GALAXIES! A dime a dozen… just one of a 100,000,000,000! 1.Galaxy Classification Ellipticals Dwarf Ellipticals Spirals Barred Spirals.
22 March 2005AST 2010: Chapter 18 1 Celestial Distances.
ASTR100 (Spring 2008) Introduction to Astronomy The Case for Dark Matter Prof. D.C. Richardson Sections
Distances. Parallax Near objects appear to move more than far objects against a distant horizon. Trigonometric parallax is used to measure distance to.
Attempts to fit/understand models: Number counts of Galaxies – Hubble,Yoshii/Peterson Angular Size Distances - distant radio cores Kellerman.
Galaxies Chapter Twenty-Six. Guiding Questions How did astronomers first discover other galaxies? How did astronomers first determine the distances to.
The Milky Way Galaxy. The Milky Way We see a band of faint light running around the entire sky. Galileo discovered it was composed of many stars. With.
The Earth-Moon-Sun System
MEASURING DISTANCE TO THE STARS
Galaxy Characteristics Surface Brightness Alternative to Luminosity I(R) = Flux/area = erg/s/cm 2 /arcsec 2 I(0) – center flux I(R) = at radius R Define.
… but the equilibrium is unstable. In order to prevent the universe from either expanding or contracting, Einstein introduced a scalar field.
Chapters 7 & 8 Rotational Motion and The Law of Gravity.
The Structure of the Universe All held together by gravitational forces.
Σπειροειδείς γαλαξίες
Galaxy Mass Star Number/Density Counting stars in a given volume
Chapter 10 Measuring the Stars. Units of Chapter 10 The Solar Neighborhood Luminosity and Apparent Brightness Stellar Temperatures Stellar Sizes The Hertzsprung-Russell.
1 Galaxies The Andromeda Galaxy - nearest galaxy similar to our own. Only 2 million light years away! Galaxies are clouds of millions to hundreds of billions.
Chapter 22 Dark Matter, Dark Energy, and the Fate of the Universe
GRAVITATIONAL LENSING
A Short Talk on… Gravitational Lensing Presented by: Anthony L, James J, and Vince V.
Exploring Dark Matter through Gravitational Lensing Exploring the Dark Universe Indiana University June 2007.
Chapter 16 Dark Matter, Dark Energy, and the Fate of the Universe.
All stars form in clouds of dust and gas. Balance of pressure: outward from core and inward from gravity.
Evidence for Stellar Evolution What proof do we have that stars evolve the way we think they do?
This page is intentionally blank. A new view of the Universe VII Fred Watson, AAO April 2005.
Chapter 7 Rotational Motion and The Law of Gravity.
Lecture Outlines Astronomy Today 7th Edition Chaisson/McMillan © 2011 Pearson Education, Inc. Chapter 23.
Space Warps. Light is believed to travel the shortest distance between two points But…… the path of light is curved in the presence of a gravitational.
Measuring the Stars Chapter Grouping of Stars Groups of stars named after animals, mythological characters, or everyday objects are called constellations.
Chapter 7 Rotational Motion and The Law of Gravity.
Objectives Determine how distances between stars are measured. Distinguish between brightness and luminosity. Identify the properties used to classify.
Cosmology and extragalactic astronomy Mat Page Mullard Space Science Lab, UCL 5. The cosmic distance ladder.
Lecture 16: Deep Space Astronomy 1143 – Spring 2014.
Astronomy 404/CSI 769 Extragalactic Astronomy
Use this loopy starter to highlight areas you need to focus on during this revision lesson. Stop the presentation after Slide 11 - Q 10. Replay at the.
Star Properties (Chapter 8). Student Learning Objectives Classify stars Explain how star properties are related.
The Mass has to do with? Mass implies light More mass, the more light. A detailed calculation shows the relation is that the Luminosity is proportional.
With measurements of true Distance, plus recessional velocity, can infer mass concentration within a given volume [us to GA] M/L ≈ M O /L O Can.
PHYS 205 Multiple Star Systems PHYS 205 Binary systems Question: Why are the binaries important?? Answer: They allow us to measure the mass of other.
Universe Tenth Edition Chapter 23 Galaxies Roger Freedman Robert Geller William Kaufmann III.
The Fate of the Universe. The fate depends on the rate of expansion and the density Density greater than critical value – gravity will halt expansion.
Chapter 7 Rotational Motion and The Law of Gravity.
Cosmology. Olbers’s Paradox The Universe may be infinite – if it is, why is the night sky dark?
Chapter 20 Cosmology. Hubble Ultra Deep Field Galaxies and Cosmology A galaxy’s age, its distance, and the age of the universe are all closely related.
Astronomical distances.
Devil physics The baddest class on campus IB Physics
Chapter 9: The Family of Stars
Chapter 14 Spiral Galaxy.
True or False: The exact length of the parametric curve {image} is {image}
True or False: The exact length of the parametric curve {image} is {image}
Presentation transcript:

Why is Rotation Speed Proportional to Mass? mv 2 /R = GMm/R 2 ; centrifugal force = gravitational force due to the mass “M” within the radius “R.” => Measure v and you produce a curve that describes v versus M

Jackson-Faber Similar to Tully-Fisher, except for Elliptical galaxies width of visible [star] light lines are the measured Refined does even better. The “fundamental plane.” Adds surface brightness of the galaxy. Plane formed from=>

Fundamental Plane Line width Luminosity Surface brightness 3 points determine a plane

Line width results from?? => The lines come from individual stars. The stars are orbiting the galaxy center that when we add up the light from all the stars

Ways to make lines broad: Intrinsic: transition rate Thermal: motion of atoms due to heat Bulk motior (needed for Jackson-Faber) => To detect it, we must have bulk motion be large enough to see “on top” of other effects

Luminosity = total intrinsic light output Surface brightness = Flux/(“solid angle”), Flux = L/4  D 2 Solid angle  r 2 /D 2, where D = the distance to the object r = the radius of the object Surface brightness is independent of distance (ignoring relativity and GR)

Measuring radius of a “fuzzy” object at a given surface brightness level good For the same objects at different distances gives the same “true” radius

Surface Brightness (the math) = (L/4  D 2 ) x 1/(  r 2 /D 2 ) = Concept different from luminosity. The key is the concept of “solid angle”  Sky patch Angle of cone => Angle area of cone =  (   Solid angle  r 2 /D 2 = solid angle =  (r/D) 2 =  (  /2) 2 r D Flux x 1/solid angle

=> Physical concept is Higher the surface brightness The better a object stands out against the background

For our small angles (less then about 1 degree),  = r/D where r = the physical [actual] radius of the object’s projected image on the sky and D = the distance to the object r D  /2 r/D = tan(  /2) sin(  /2)  /2 in radians 1 radian = degrees

Example: tan(1 degree) = sin(1 degree) = / = => Good to 4 decimal places, which is good enough If you don’t have a calculator handy, use 1 radian 60 degrees.

Fundamental Plane Example of cross calibration: FLUXFLUX Sur. Br x Line Width * Measured Then measure D by Cepheids. => *Real formula is more complex.

Fundamental Plane Example of cross calibration: LuminosityLuminosity Sur. Br x Line Width Derived Now luminosity; with L = F x 4  D 2

Fundamental Plane Measure surface brightness and line width, Derive L Also measure F then derive D or

Other methods: Other (besides Cepheids and SNeIa) standard candles

Globular Clusters and Brightest Cluster Galaxy use two concepts: There is maximum size to things: The largest globular cluster in a galaxy or The largest galaxy in a cluster Are always about the same size. Total mass and total light (luminosity) are directly related. Standard Candle

What is a globular cluster? M2 has a diameter of about 140 light-years (47 pc), contains about 150,000 stars, (You already know about clusters of galaxies)

Other methods: (1) Gravitational Lenses: Delay in the travel time over one path vs another Dependent on the true path length Measure distances this way. (2) The S-Z (Sunyaev-Zel’dovich Effect): Interaction of the hot gas with the CMB Effect depends on the true size of the cluster Plus model of the gas temperature profile.

GR lens Concept: “false” = “lensed image” True image If “ a” varies we’ll see “b” vary exactly the same way later. Measure time delay =  =  /c where  = (  )- , use trig. to calculate  measure v, derive H 0 a b  observer

Problems with Grav. lens hard to correlate the variability of the images since the object varies randomly we need to model the mass distribution of the lens to derive the path length (c ) there aren’t many of these systems, and they are difficult to identify. Identification requires demonstrating the two (really many, but we’re keeping it simple) images you detect are from the same “true” object and not a chance “coincidence”

Typical separations are a few arc seconds. Remember 1 degree = 60 arc minutes; 1 arc minute = 60 arc seconds => 1 degree = 3600 arc seconds. An abnormally high gravitational field can cause a path deflection that corresponds to an arc minute or more => About 15 years ago, astronomers in a prestigious eastern school found two images that appeared to come from the same object and were separated by nearly 2 arc minutes=>

They concluded that they’d detected something unusual called a “cosmic” string” => 15 minutes of fame Until an astronomer at another [competing] prestigious eastern university showed that this was a chance coincidence of two similar looking objects If we ever discover a cosmic string this will be very exciting. This discovery would show that “defects in space” can really exist!